The MDI model, that combines both density and momentum dependent interaction among the nucleons, is suitable for studying neutron star matter at zero (present study) as well as at finite temperature. In particular, although it was introduced by Gale et al. [1]}, [2]} to examine the influence of momentum dependent interactions on the momentum flow of heavy-ion collisions, the model has been modified, elaborated, and applied also in the study of the properties of nuclear matter at neutron stars. The advantages of the MDI model are: (a) reproduces with high accuracy the properties of SNM at the saturation density, including isovector quantities, (b) reproduces the microscopic properties of the Chiral model for pure neutron matter and the results of state-of-the-art calculations of Akmal et al. [3]}, (c) predicts maximum neutron star mass higher than the observed ones [4]}, [5]}, [6]}, and (d) maintains the causal behavior of the EoS even at densities higher than the ones at the maximum mass configuration.
